J2345-0449

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J2345-0449
SDSS image of J2345-0449.jpg
SDSS image of J2345-0449
Observation data (J2000 epoch)
Constellation Aquarius
Right ascension 23h 45m 32.70s
Declination −04° 49′ 25.4″
Redshift 0.075566
Heliocentric radial velocity 22,654 km/s
Distance 947 Mly (290.3 Mpc)
Apparent magnitude  (V)0.086
Apparent magnitude  (B)0.113
Surface brightness 16.19
Characteristics
Apparent size  (V)0.62' x 0.31'
Notable featuresOne of the most massive spiral galaxies containing a radio jet
Other designations
PGC 1052974, GRS J2345-0449, 2MASX J23453268-0449256, 6dF J2345327-044925

J2345-0449 or 2MASX J23453268-0449256, is a spiral galaxy located 947 million light-years in the constellation of Aquarius. [1] It contains an active galactic nucleus and is classified as a radio galaxy, containing relativistic jets that are projected out from its spiral host by ~1.6 Mpc, making these jets the largest and rarest known. [2] [3] It was discovered in 2014 by amateur astronomers, making it the third spiral DRAGN after ESO 0313-192 and Speca. [2]

Contents

Physical Properties

Mentioned as a megaparsec-scale object at redshift 0.0757, [4] J2345-0449 is one of the massive spiral galaxies found in the universe. [5] [6] It is also one of the largest radio sources discovered since the galaxy exhibits two sets of radio lobes found in near alignment and spanning a width of ∼387.2 kpc (∼452) and ∼1.63 Mpc (∼191). [2] According to Very Large Array 6 cm imaging, the inner radio lobes are categorized either Fanaroff-Riley Class I or FR II morphology. [7]

J2345-0449 contains a fast rotation speed of Vrot = 371/sin (i) = 429 ± 30 km s−1 that is r ≥ 10 kpc away from its galactic center. [8] It has a mass of Mstellar = 4 × 1011 M⊙ and a surrounding ring of molecular gas measured 24 kpc wide in diameter. The galaxy has a star formation rate with a surface density measured to be ΣSFR = 1.8 × 10−3 M⊙ yr−1 kpc−2. [9] However it has a low factor between 30 and 70 as expected according to the Kennicutt-Schmidt law. [10]

Black hole mass of J2345-0449

The black hole mass estimation is challenging since J2345-0449 has no classic bulge structure. According to Bagchi, the black hole has a mass of 2.5 ± 0.5 × 108 M⊙. Further observations shows it has a mass of 1.4× 109 M⊙ when calculating the MBH–σ relation proposed by Gültekin. [11] However, according to researchers obtaining the M–σ relation from McConnell & Ma, [12] the actual mass of J2345-0449 is 5 × 109 M⊙. [8]

Related Research Articles

An active galactic nucleus (AGN) is a compact region at the center of a galaxy that emits a significant amount of energy across the electromagnetic spectrum, with characteristics indicating that this luminosity is not produced by the stars. Such excess, non-stellar emissions have been observed in the radio, microwave, infrared, optical, ultra-violet, X-ray and gamma ray wavebands. A galaxy hosting an AGN is called an active galaxy. The non-stellar radiation from an AGN is theorized to result from the accretion of matter by a supermassive black hole at the center of its host galaxy.

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<span class="mw-page-title-main">RX J1532.9+3021</span> Galaxy cluster in the constellation Corona Borealis

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NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 Seyfert galaxy.

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<span class="mw-page-title-main">NGC 4294</span> Galaxy in the constellation Virgo

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<span class="mw-page-title-main">4C +29.30</span> Galaxy in the constellation Cancer

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<span class="mw-page-title-main">MRC 0406-244</span> Radio galaxy producing an astrophysical jet in the constellation of Eridanus

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MRC 2011-298 is an elliptical galaxy with an active galactic nucleus, located in the constellation of Sagittarius. It is located 2.1 billion light-years away from Earth. MRC 2011-298 is the brightest cluster galaxy in the galaxy cluster, Abell 3670 and classfied as a dumbbell galaxy, an optical system with two galactic nuclei separated by 7″, corresponding to ≃17 kpc according to the adopted cosmology, with similar magnitude and a common stellar halo. The galaxy is known to have an ellipticity of ε = 0.28 and a position angle of PA  =  24° that is measured from north to east.

<span class="mw-page-title-main">4C +72.26</span> Radio galaxy in the constellation Draco

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References

  1. ↑ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-07-16.
  2. 1 2 3 Bagchi, Joydeep; Vivek, M.; Vikram, Vinu; Hota, Ananda; Biju, K. G.; Sirothia, S. K.; Srianand, Raghunathan; Gopal-Krishna; Jacob, Joe (2014-06-05). "Megaparsec Relativistic Jets Launched from an Accreting Supermassive Black Hole in an Extreme Spiral Galaxy". The Astrophysical Journal. 788 (2): 174. doi:10.1088/0004-637x/788/2/174. ISSN   0004-637X.
  3. ↑ Walker, Stephen (2013-09-01). "Detecting the hot gaseous halo around an extremely massive and relativistic jet launching spiral galaxy". Chandra Proposal: 3824. Bibcode:2013cxo..prop.3824W.
  4. ↑ Machalski, J.; Koziel-Wierzbowska, D.; Jamrozy, M. (2007-10-24), Giant Radio Galaxies as a probe of the cosmological evolution of the IGM, I. Preliminary deep detections and low-resolution spectroscopy with the SALT, arXiv: 0710.4512
  5. ↑ Posti, Lorenzo; Fraternali, Filippo; Marasco, Antonino (2019-06-01). "Peak star formation efficiency and no missing baryons in massive spirals". Astronomy and Astrophysics. 626: A56. arXiv: 1812.05099 . Bibcode:2019A&A...626A..56P. doi:10.1051/0004-6361/201935553. ISSN   0004-6361.
  6. ↑ Bagchi, Joydeep; Ray, Shankar; Dhiwar, Suraj; Dabhade, Pratik; Barth, Aaron; Ho, Luis C.; Mirakhor, Mohammad S.; Walker, Stephen A.; Nesvadba, Nicole (2024-05-03), Unveiling the Bulge-Disc Structure, AGN Feedback, and Baryon Landscape in a Massive Spiral Galaxy with Mpc-Scale Radio Jets, arXiv: 2405.01910 , retrieved 2024-07-16
  7. ↑ Parma, P. (1982), "Westerbork Observations of Low Luminosity Radio Sources", Extragalactic Radio Sources, Dordrecht: Springer Netherlands, pp. 193–194, doi:10.1007/978-94-009-7781-5_55, ISBN   978-94-009-7783-9 , retrieved 2024-07-16
  8. 1 2 Walker, S. A.; Bagchi, J.; Fabian, A. C. (2015-04-09). "A deep Chandra observation of the hot gaseous halo around a rare, extremely massive and relativistic jet launching spiral galaxy". Monthly Notices of the Royal Astronomical Society. 449 (4): 3527–3534. doi: 10.1093/mnras/stv616 . ISSN   0035-8711.
  9. ↑ Nesvadba, N. P. H.; Wagner, A. Y.; Mukherjee, D.; Mandal, A.; Janssen, R. M. J.; Zovaro, H.; Neumayer, N.; Bagchi, J.; Bicknell, G. (2021-10-01). "Jet-driven AGN feedback on molecular gas and low star-formation efficiency in a massive local spiral galaxy with a bright X-ray halo". Astronomy & Astrophysics. 654: A8. doi:10.1051/0004-6361/202140544. ISSN   0004-6361.
  10. ↑ Drevet Mulard, M.; Nesvadba, N. P. H.; Meenakshi, M.; Mukherjee, D.; Wagner, A.; Bicknell, G.; Neumayer, N.; Combes, F.; Zovaro, H.; Janssen, R. M. J.; Bagchi, J.; Dabhade, P.; Prunet, S. (2023-08-01). "Star formation in a massive spiral galaxy with a radio-AGN". Astronomy and Astrophysics. 676: A35. Bibcode:2023A&A...676A..35D. doi:10.1051/0004-6361/202245173. ISSN   0004-6361.
  11. ↑ Gültekin, Kayhan; Cackett, Edward M.; Miller, Jon M.; Di Matteo, Tiziana; Markoff, Sera; Richstone, Douglas O. (2009-11-01). "The Fundamental Plane of Accretion onto Black Holes with Dynamical Masses". The Astrophysical Journal. 706 (1): 404–416. arXiv: 0906.3285 . Bibcode:2009ApJ...706..404G. doi:10.1088/0004-637X/706/1/404. ISSN   0004-637X.
  12. ↑ McConnell, Nicholas J.; Ma, Chung-Pei (2013-02-01). "Revisiting the Scaling Relations of Black Hole Masses and Host Galaxy Properties". The Astrophysical Journal. 764 (2): 184. arXiv: 1211.2816 . Bibcode:2013ApJ...764..184M. doi:10.1088/0004-637X/764/2/184. ISSN   0004-637X.
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